[Okc-wp4] EO meeting 23rd of February

[Haakon Andresen]

Reminder, today at 13:00.

Our speaker today will join us remotely, so feel free to join in person in A5:1003 or zoom in.

________________________________
From: Okc-wp4-at-fysik.su.se <okc-wp4-at-fysik.su.se-bounces at lists.su.se> on behalf of Haakon Andresen via Okc-wp4-at-fysik.su.se <okc-wp4-at-fysik.su.se at lists.su.se>
Sent: 20 February 2023 11:40:25
To: Okc-wp4 at fysik.su.se
Cc: Ricard Aguilera Miret
Subject: [Okc-wp4] EO meeting 23rd of February


Dear everyone,

This weeks EO seminar will be given by Ricard Aguilera Miret, who will talk about "Turbulent magnetic field amplification in BNS mergers".
Our usual room has been booked by someone else and we will therefore meet at 13:00 in A5:1003.

Our speaker will join us remotely and we will use the following zoom link https://stockholmuniversity.zoom.us/j/62363340520

Best,
Haakon (on behalf of the EO seminar organizers)

When: 23rd of February, 13:00
Where: A5:1003, https://stockholmuniversity.zoom.us/j/62363340520

Speaker: Ricard Aguilera Miret
Title: Turbulent magnetic field amplification in BNS mergers

Abstract
The detection of a binary neutron star merger in 2017 through both
gravitational waves and electromagnetic emission opened a new era of
multimessenger astronomy. During the merger, several mechanisms like the
Kelvin-Helmholtz instability, the winding up effect and the MRI, can
amplify the initial magnetic field in the remnant to be powerful enoguh
for launching a jet, with an associated short GRB. When performing
simulations, simplified assumptions arise for the initial magnetic field
strength and topology of the merging neutron stars. Here I will show
convergent results by using high-resolution, large-eddy simulations of
binary neutron star mergers, following the newly formed remnant for up
to 30 milliseconds. I will specifically compare simulations with
different initial magnetic field strenghts and configurations, going
beyond the widespread-used aligned dipole confined within each star. I
will show that the magnetic field is always amplified up to ~10^16 G in
the bulk region of the remnant, while the initial topology is quickly
forgotten in a timescale of few miliseconds after the merger due to the
Kelvin-Helmholtz instability.

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